NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts
Aims. Deep millimeter surveys are necessary to probe the dust-obscured galaxies at high redshift. We conducted a large observing program at 1.2 and 2 mm with the NIKA2 camera installed on the IRAM 30-meter telescope. This NIKA2 Cosmological Legacy Survey (N2CLS) covers two emblematic fields: GOODS-N...
Gespeichert in:
| Veröffentlicht in: | arXiv.org 2023-05 |
|---|---|
| Hauptverfasser: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | |
|---|---|
| container_issue | |
| container_start_page | |
| container_title | arXiv.org |
| container_volume | |
| creator | Bing, L Béthermin, M Lagache, G Adam, R Ade, P Ajeddig, H André, P Artis, E Aussel, H Beelen, A Benoît, A Berta, S Billot, N Bourrion, O Calvo, M Catalano, A De Petris, M Désert, F -X Doyle, S Driessen, E F C Elbaz, D Gkogkou, A Gomez, A Goupy, J Hanser, C Kéruzoré, F Kramer, C Ladjelate, B Liu, D Leclercq, S J -F Lestrade Lustig, P Macías-Pérez, J F Maury, A Mauskopf, P Mayet, F Monfardini, A Muñoz-Echeverría, M Perotto, L Pisano, G Ponthieu, N Revéret, V Rigby, A J Ritacco, A Romero, C Roussel, H Ruppin, F Schuster, K Sievers, A Tucker, C Zylka, R |
| description | Aims. Deep millimeter surveys are necessary to probe the dust-obscured galaxies at high redshift. We conducted a large observing program at 1.2 and 2 mm with the NIKA2 camera installed on the IRAM 30-meter telescope. This NIKA2 Cosmological Legacy Survey (N2CLS) covers two emblematic fields: GOODS-N and COSMOS. We introduce the N2CLS survey and present new 1.2 and 2 mm number count measurements based on the tiered N2CLS observations from October 2017 to May 2021. Methods. We develop an end-to-end simulation that combines an input sky model with the instrument noise and data reduction pipeline artifacts. This simulation is used to compute the sample purity, flux boosting, pipeline transfer function, completeness, and effective area of the survey. We used the 117 deg\(^2\) SIDES simulations as the sky model, which include the galaxy clustering. Our formalism allows us to correct the source number counts to obtain galaxy number counts, the difference between the two being due to resolution effects caused by the blending of several galaxies inside the large beam of single-dish instruments. Results. The N2CLS-May2021 survey reaches an average 1-\(\sigma\) noise level of 0.17 and 0.048 mJy on GOODS-N over 159 arcmin\(^2\), and 0.46 and 0.14 mJy on COSMOS over 1010 arcmin\(^2\), at 1.2 and 2 mm, respectively. For a purity threshold of 80%, we detect 120 and 67 sources in GOODS-N and 195 and 76 sources in COSMOS, at 1.2 and 2 mm, respectively. Our measurement connects the bright single-dish to the deep interferometric number counts. After correcting for resolution effects, our results reconcile the single-dish and interferometric number counts and are further accurately compared with model predictions. |
| doi_str_mv | 10.48550/arxiv.2305.07054 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_arxiv</sourceid><recordid>TN_cdi_arxiv_primary_2305_07054</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2813744385</sourcerecordid><originalsourceid>FETCH-LOGICAL-a525-39c04e728a62cca8508a635ac1c1efc0c9de2d426779c919f08e4f66b86b9e403</originalsourceid><addsrcrecordid>eNotj09PgzAchhsTE5e5D-DJJp7BH_0DrbcFdS7iPLg7KaUsLECxHcv49uK20_se3jx5H4QeIgiZ4ByelTvVx5BQ4CEkwNkNmhFKo0AwQu7Qwvs9AJA4IZzTGfrarD-XBKfWt7axu1qrBmdmp_SIfwZ3NOPLNfGr8drV_aG2HVZdiVeqUacRb4a2MG4CDN3B36PbSjXeLK45R9v3t236EWTfq3W6zALFCQ-o1MBMQoSKidZKcJga5UpHOjKVBi1LQ0o2fUyklpGsQBhWxXEh4kIaBnSOHi_Ys2veu7pVbsz_nfOz87R4uix6Z38H4w_53g6umz7lREQ0YYwKTv8AadFYvA</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2813744385</pqid></control><display><type>article</type><title>NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Bing, L ; Béthermin, M ; Lagache, G ; Adam, R ; Ade, P ; Ajeddig, H ; André, P ; Artis, E ; Aussel, H ; Beelen, A ; Benoît, A ; Berta, S ; Billot, N ; Bourrion, O ; Calvo, M ; Catalano, A ; De Petris, M ; Désert, F -X ; Doyle, S ; Driessen, E F C ; Elbaz, D ; Gkogkou, A ; Gomez, A ; Goupy, J ; Hanser, C ; Kéruzoré, F ; Kramer, C ; Ladjelate, B ; Liu, D ; Leclercq, S ; J -F Lestrade ; Lustig, P ; Macías-Pérez, J F ; Maury, A ; Mauskopf, P ; Mayet, F ; Monfardini, A ; Muñoz-Echeverría, M ; Perotto, L ; Pisano, G ; Ponthieu, N ; Revéret, V ; Rigby, A J ; Ritacco, A ; Romero, C ; Roussel, H ; Ruppin, F ; Schuster, K ; Sievers, A ; Tucker, C ; Zylka, R</creator><creatorcontrib>Bing, L ; Béthermin, M ; Lagache, G ; Adam, R ; Ade, P ; Ajeddig, H ; André, P ; Artis, E ; Aussel, H ; Beelen, A ; Benoît, A ; Berta, S ; Billot, N ; Bourrion, O ; Calvo, M ; Catalano, A ; De Petris, M ; Désert, F -X ; Doyle, S ; Driessen, E F C ; Elbaz, D ; Gkogkou, A ; Gomez, A ; Goupy, J ; Hanser, C ; Kéruzoré, F ; Kramer, C ; Ladjelate, B ; Liu, D ; Leclercq, S ; J -F Lestrade ; Lustig, P ; Macías-Pérez, J F ; Maury, A ; Mauskopf, P ; Mayet, F ; Monfardini, A ; Muñoz-Echeverría, M ; Perotto, L ; Pisano, G ; Ponthieu, N ; Revéret, V ; Rigby, A J ; Ritacco, A ; Romero, C ; Roussel, H ; Ruppin, F ; Schuster, K ; Sievers, A ; Tucker, C ; Zylka, R</creatorcontrib><description>Aims. Deep millimeter surveys are necessary to probe the dust-obscured galaxies at high redshift. We conducted a large observing program at 1.2 and 2 mm with the NIKA2 camera installed on the IRAM 30-meter telescope. This NIKA2 Cosmological Legacy Survey (N2CLS) covers two emblematic fields: GOODS-N and COSMOS. We introduce the N2CLS survey and present new 1.2 and 2 mm number count measurements based on the tiered N2CLS observations from October 2017 to May 2021. Methods. We develop an end-to-end simulation that combines an input sky model with the instrument noise and data reduction pipeline artifacts. This simulation is used to compute the sample purity, flux boosting, pipeline transfer function, completeness, and effective area of the survey. We used the 117 deg\(^2\) SIDES simulations as the sky model, which include the galaxy clustering. Our formalism allows us to correct the source number counts to obtain galaxy number counts, the difference between the two being due to resolution effects caused by the blending of several galaxies inside the large beam of single-dish instruments. Results. The N2CLS-May2021 survey reaches an average 1-\(\sigma\) noise level of 0.17 and 0.048 mJy on GOODS-N over 159 arcmin\(^2\), and 0.46 and 0.14 mJy on COSMOS over 1010 arcmin\(^2\), at 1.2 and 2 mm, respectively. For a purity threshold of 80%, we detect 120 and 67 sources in GOODS-N and 195 and 76 sources in COSMOS, at 1.2 and 2 mm, respectively. Our measurement connects the bright single-dish to the deep interferometric number counts. After correcting for resolution effects, our results reconcile the single-dish and interferometric number counts and are further accurately compared with model predictions.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2305.07054</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Blending effects ; Clustering ; Cosmic dust ; Cosmos ; Galaxies ; Interferometry ; Noise levels ; Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Physics - Instrumentation and Methods for Astrophysics ; Purity ; Red shift ; Simulation ; Sky models ; Sky surveys (astronomy) ; Stars & galaxies ; Transfer functions</subject><ispartof>arXiv.org, 2023-05</ispartof><rights>2023. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2305.07054$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1051/0004-6361/202346579$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Bing, L</creatorcontrib><creatorcontrib>Béthermin, M</creatorcontrib><creatorcontrib>Lagache, G</creatorcontrib><creatorcontrib>Adam, R</creatorcontrib><creatorcontrib>Ade, P</creatorcontrib><creatorcontrib>Ajeddig, H</creatorcontrib><creatorcontrib>André, P</creatorcontrib><creatorcontrib>Artis, E</creatorcontrib><creatorcontrib>Aussel, H</creatorcontrib><creatorcontrib>Beelen, A</creatorcontrib><creatorcontrib>Benoît, A</creatorcontrib><creatorcontrib>Berta, S</creatorcontrib><creatorcontrib>Billot, N</creatorcontrib><creatorcontrib>Bourrion, O</creatorcontrib><creatorcontrib>Calvo, M</creatorcontrib><creatorcontrib>Catalano, A</creatorcontrib><creatorcontrib>De Petris, M</creatorcontrib><creatorcontrib>Désert, F -X</creatorcontrib><creatorcontrib>Doyle, S</creatorcontrib><creatorcontrib>Driessen, E F C</creatorcontrib><creatorcontrib>Elbaz, D</creatorcontrib><creatorcontrib>Gkogkou, A</creatorcontrib><creatorcontrib>Gomez, A</creatorcontrib><creatorcontrib>Goupy, J</creatorcontrib><creatorcontrib>Hanser, C</creatorcontrib><creatorcontrib>Kéruzoré, F</creatorcontrib><creatorcontrib>Kramer, C</creatorcontrib><creatorcontrib>Ladjelate, B</creatorcontrib><creatorcontrib>Liu, D</creatorcontrib><creatorcontrib>Leclercq, S</creatorcontrib><creatorcontrib>J -F Lestrade</creatorcontrib><creatorcontrib>Lustig, P</creatorcontrib><creatorcontrib>Macías-Pérez, J F</creatorcontrib><creatorcontrib>Maury, A</creatorcontrib><creatorcontrib>Mauskopf, P</creatorcontrib><creatorcontrib>Mayet, F</creatorcontrib><creatorcontrib>Monfardini, A</creatorcontrib><creatorcontrib>Muñoz-Echeverría, M</creatorcontrib><creatorcontrib>Perotto, L</creatorcontrib><creatorcontrib>Pisano, G</creatorcontrib><creatorcontrib>Ponthieu, N</creatorcontrib><creatorcontrib>Revéret, V</creatorcontrib><creatorcontrib>Rigby, A J</creatorcontrib><creatorcontrib>Ritacco, A</creatorcontrib><creatorcontrib>Romero, C</creatorcontrib><creatorcontrib>Roussel, H</creatorcontrib><creatorcontrib>Ruppin, F</creatorcontrib><creatorcontrib>Schuster, K</creatorcontrib><creatorcontrib>Sievers, A</creatorcontrib><creatorcontrib>Tucker, C</creatorcontrib><creatorcontrib>Zylka, R</creatorcontrib><title>NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts</title><title>arXiv.org</title><description>Aims. Deep millimeter surveys are necessary to probe the dust-obscured galaxies at high redshift. We conducted a large observing program at 1.2 and 2 mm with the NIKA2 camera installed on the IRAM 30-meter telescope. This NIKA2 Cosmological Legacy Survey (N2CLS) covers two emblematic fields: GOODS-N and COSMOS. We introduce the N2CLS survey and present new 1.2 and 2 mm number count measurements based on the tiered N2CLS observations from October 2017 to May 2021. Methods. We develop an end-to-end simulation that combines an input sky model with the instrument noise and data reduction pipeline artifacts. This simulation is used to compute the sample purity, flux boosting, pipeline transfer function, completeness, and effective area of the survey. We used the 117 deg\(^2\) SIDES simulations as the sky model, which include the galaxy clustering. Our formalism allows us to correct the source number counts to obtain galaxy number counts, the difference between the two being due to resolution effects caused by the blending of several galaxies inside the large beam of single-dish instruments. Results. The N2CLS-May2021 survey reaches an average 1-\(\sigma\) noise level of 0.17 and 0.048 mJy on GOODS-N over 159 arcmin\(^2\), and 0.46 and 0.14 mJy on COSMOS over 1010 arcmin\(^2\), at 1.2 and 2 mm, respectively. For a purity threshold of 80%, we detect 120 and 67 sources in GOODS-N and 195 and 76 sources in COSMOS, at 1.2 and 2 mm, respectively. Our measurement connects the bright single-dish to the deep interferometric number counts. After correcting for resolution effects, our results reconcile the single-dish and interferometric number counts and are further accurately compared with model predictions.</description><subject>Blending effects</subject><subject>Clustering</subject><subject>Cosmic dust</subject><subject>Cosmos</subject><subject>Galaxies</subject><subject>Interferometry</subject><subject>Noise levels</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Purity</subject><subject>Red shift</subject><subject>Simulation</subject><subject>Sky models</subject><subject>Sky surveys (astronomy)</subject><subject>Stars & galaxies</subject><subject>Transfer functions</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj09PgzAchhsTE5e5D-DJJp7BH_0DrbcFdS7iPLg7KaUsLECxHcv49uK20_se3jx5H4QeIgiZ4ByelTvVx5BQ4CEkwNkNmhFKo0AwQu7Qwvs9AJA4IZzTGfrarD-XBKfWt7axu1qrBmdmp_SIfwZ3NOPLNfGr8drV_aG2HVZdiVeqUacRb4a2MG4CDN3B36PbSjXeLK45R9v3t236EWTfq3W6zALFCQ-o1MBMQoSKidZKcJga5UpHOjKVBi1LQ0o2fUyklpGsQBhWxXEh4kIaBnSOHi_Ys2veu7pVbsz_nfOz87R4uix6Z38H4w_53g6umz7lREQ0YYwKTv8AadFYvA</recordid><startdate>20230511</startdate><enddate>20230511</enddate><creator>Bing, L</creator><creator>Béthermin, M</creator><creator>Lagache, G</creator><creator>Adam, R</creator><creator>Ade, P</creator><creator>Ajeddig, H</creator><creator>André, P</creator><creator>Artis, E</creator><creator>Aussel, H</creator><creator>Beelen, A</creator><creator>Benoît, A</creator><creator>Berta, S</creator><creator>Billot, N</creator><creator>Bourrion, O</creator><creator>Calvo, M</creator><creator>Catalano, A</creator><creator>De Petris, M</creator><creator>Désert, F -X</creator><creator>Doyle, S</creator><creator>Driessen, E F C</creator><creator>Elbaz, D</creator><creator>Gkogkou, A</creator><creator>Gomez, A</creator><creator>Goupy, J</creator><creator>Hanser, C</creator><creator>Kéruzoré, F</creator><creator>Kramer, C</creator><creator>Ladjelate, B</creator><creator>Liu, D</creator><creator>Leclercq, S</creator><creator>J -F Lestrade</creator><creator>Lustig, P</creator><creator>Macías-Pérez, J F</creator><creator>Maury, A</creator><creator>Mauskopf, P</creator><creator>Mayet, F</creator><creator>Monfardini, A</creator><creator>Muñoz-Echeverría, M</creator><creator>Perotto, L</creator><creator>Pisano, G</creator><creator>Ponthieu, N</creator><creator>Revéret, V</creator><creator>Rigby, A J</creator><creator>Ritacco, A</creator><creator>Romero, C</creator><creator>Roussel, H</creator><creator>Ruppin, F</creator><creator>Schuster, K</creator><creator>Sievers, A</creator><creator>Tucker, C</creator><creator>Zylka, R</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20230511</creationdate><title>NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts</title><author>Bing, L ; Béthermin, M ; Lagache, G ; Adam, R ; Ade, P ; Ajeddig, H ; André, P ; Artis, E ; Aussel, H ; Beelen, A ; Benoît, A ; Berta, S ; Billot, N ; Bourrion, O ; Calvo, M ; Catalano, A ; De Petris, M ; Désert, F -X ; Doyle, S ; Driessen, E F C ; Elbaz, D ; Gkogkou, A ; Gomez, A ; Goupy, J ; Hanser, C ; Kéruzoré, F ; Kramer, C ; Ladjelate, B ; Liu, D ; Leclercq, S ; J -F Lestrade ; Lustig, P ; Macías-Pérez, J F ; Maury, A ; Mauskopf, P ; Mayet, F ; Monfardini, A ; Muñoz-Echeverría, M ; Perotto, L ; Pisano, G ; Ponthieu, N ; Revéret, V ; Rigby, A J ; Ritacco, A ; Romero, C ; Roussel, H ; Ruppin, F ; Schuster, K ; Sievers, A ; Tucker, C ; Zylka, R</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a525-39c04e728a62cca8508a635ac1c1efc0c9de2d426779c919f08e4f66b86b9e403</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Blending effects</topic><topic>Clustering</topic><topic>Cosmic dust</topic><topic>Cosmos</topic><topic>Galaxies</topic><topic>Interferometry</topic><topic>Noise levels</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Purity</topic><topic>Red shift</topic><topic>Simulation</topic><topic>Sky models</topic><topic>Sky surveys (astronomy)</topic><topic>Stars & galaxies</topic><topic>Transfer functions</topic><toplevel>online_resources</toplevel><creatorcontrib>Bing, L</creatorcontrib><creatorcontrib>Béthermin, M</creatorcontrib><creatorcontrib>Lagache, G</creatorcontrib><creatorcontrib>Adam, R</creatorcontrib><creatorcontrib>Ade, P</creatorcontrib><creatorcontrib>Ajeddig, H</creatorcontrib><creatorcontrib>André, P</creatorcontrib><creatorcontrib>Artis, E</creatorcontrib><creatorcontrib>Aussel, H</creatorcontrib><creatorcontrib>Beelen, A</creatorcontrib><creatorcontrib>Benoît, A</creatorcontrib><creatorcontrib>Berta, S</creatorcontrib><creatorcontrib>Billot, N</creatorcontrib><creatorcontrib>Bourrion, O</creatorcontrib><creatorcontrib>Calvo, M</creatorcontrib><creatorcontrib>Catalano, A</creatorcontrib><creatorcontrib>De Petris, M</creatorcontrib><creatorcontrib>Désert, F -X</creatorcontrib><creatorcontrib>Doyle, S</creatorcontrib><creatorcontrib>Driessen, E F C</creatorcontrib><creatorcontrib>Elbaz, D</creatorcontrib><creatorcontrib>Gkogkou, A</creatorcontrib><creatorcontrib>Gomez, A</creatorcontrib><creatorcontrib>Goupy, J</creatorcontrib><creatorcontrib>Hanser, C</creatorcontrib><creatorcontrib>Kéruzoré, F</creatorcontrib><creatorcontrib>Kramer, C</creatorcontrib><creatorcontrib>Ladjelate, B</creatorcontrib><creatorcontrib>Liu, D</creatorcontrib><creatorcontrib>Leclercq, S</creatorcontrib><creatorcontrib>J -F Lestrade</creatorcontrib><creatorcontrib>Lustig, P</creatorcontrib><creatorcontrib>Macías-Pérez, J F</creatorcontrib><creatorcontrib>Maury, A</creatorcontrib><creatorcontrib>Mauskopf, P</creatorcontrib><creatorcontrib>Mayet, F</creatorcontrib><creatorcontrib>Monfardini, A</creatorcontrib><creatorcontrib>Muñoz-Echeverría, M</creatorcontrib><creatorcontrib>Perotto, L</creatorcontrib><creatorcontrib>Pisano, G</creatorcontrib><creatorcontrib>Ponthieu, N</creatorcontrib><creatorcontrib>Revéret, V</creatorcontrib><creatorcontrib>Rigby, A J</creatorcontrib><creatorcontrib>Ritacco, A</creatorcontrib><creatorcontrib>Romero, C</creatorcontrib><creatorcontrib>Roussel, H</creatorcontrib><creatorcontrib>Ruppin, F</creatorcontrib><creatorcontrib>Schuster, K</creatorcontrib><creatorcontrib>Sievers, A</creatorcontrib><creatorcontrib>Tucker, C</creatorcontrib><creatorcontrib>Zylka, R</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bing, L</au><au>Béthermin, M</au><au>Lagache, G</au><au>Adam, R</au><au>Ade, P</au><au>Ajeddig, H</au><au>André, P</au><au>Artis, E</au><au>Aussel, H</au><au>Beelen, A</au><au>Benoît, A</au><au>Berta, S</au><au>Billot, N</au><au>Bourrion, O</au><au>Calvo, M</au><au>Catalano, A</au><au>De Petris, M</au><au>Désert, F -X</au><au>Doyle, S</au><au>Driessen, E F C</au><au>Elbaz, D</au><au>Gkogkou, A</au><au>Gomez, A</au><au>Goupy, J</au><au>Hanser, C</au><au>Kéruzoré, F</au><au>Kramer, C</au><au>Ladjelate, B</au><au>Liu, D</au><au>Leclercq, S</au><au>J -F Lestrade</au><au>Lustig, P</au><au>Macías-Pérez, J F</au><au>Maury, A</au><au>Mauskopf, P</au><au>Mayet, F</au><au>Monfardini, A</au><au>Muñoz-Echeverría, M</au><au>Perotto, L</au><au>Pisano, G</au><au>Ponthieu, N</au><au>Revéret, V</au><au>Rigby, A J</au><au>Ritacco, A</au><au>Romero, C</au><au>Roussel, H</au><au>Ruppin, F</au><au>Schuster, K</au><au>Sievers, A</au><au>Tucker, C</au><au>Zylka, R</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts</atitle><jtitle>arXiv.org</jtitle><date>2023-05-11</date><risdate>2023</risdate><eissn>2331-8422</eissn><abstract>Aims. Deep millimeter surveys are necessary to probe the dust-obscured galaxies at high redshift. We conducted a large observing program at 1.2 and 2 mm with the NIKA2 camera installed on the IRAM 30-meter telescope. This NIKA2 Cosmological Legacy Survey (N2CLS) covers two emblematic fields: GOODS-N and COSMOS. We introduce the N2CLS survey and present new 1.2 and 2 mm number count measurements based on the tiered N2CLS observations from October 2017 to May 2021. Methods. We develop an end-to-end simulation that combines an input sky model with the instrument noise and data reduction pipeline artifacts. This simulation is used to compute the sample purity, flux boosting, pipeline transfer function, completeness, and effective area of the survey. We used the 117 deg\(^2\) SIDES simulations as the sky model, which include the galaxy clustering. Our formalism allows us to correct the source number counts to obtain galaxy number counts, the difference between the two being due to resolution effects caused by the blending of several galaxies inside the large beam of single-dish instruments. Results. The N2CLS-May2021 survey reaches an average 1-\(\sigma\) noise level of 0.17 and 0.048 mJy on GOODS-N over 159 arcmin\(^2\), and 0.46 and 0.14 mJy on COSMOS over 1010 arcmin\(^2\), at 1.2 and 2 mm, respectively. For a purity threshold of 80%, we detect 120 and 67 sources in GOODS-N and 195 and 76 sources in COSMOS, at 1.2 and 2 mm, respectively. Our measurement connects the bright single-dish to the deep interferometric number counts. After correcting for resolution effects, our results reconcile the single-dish and interferometric number counts and are further accurately compared with model predictions.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2305.07054</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2023-05 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_2305_07054 |
| source | arXiv.org; Free E- Journals |
| subjects | Blending effects Clustering Cosmic dust Cosmos Galaxies Interferometry Noise levels Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Instrumentation and Methods for Astrophysics Purity Red shift Simulation Sky models Sky surveys (astronomy) Stars & galaxies Transfer functions |
| title | NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-06T17%3A55%3A33IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=NIKA2%20Cosmological%20Legacy%20Survey:%20Survey%20Description%20and%20Galaxy%20Number%20Counts&rft.jtitle=arXiv.org&rft.au=Bing,%20L&rft.date=2023-05-11&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2305.07054&rft_dat=%3Cproquest_arxiv%3E2813744385%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2813744385&rft_id=info:pmid/&rfr_iscdi=true |